DOCSLIB.ORG

Subaru and Roman Space Telescope

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Subaru and Roman Space Telescope Goal: l share Roman status l share Synergistic observation status l Discussion • Compatibility with PFS SSP after 2027 • Balance of Dark/Bright night • Front-loading • Expanding Keck exchange time? <agenda> Roman Status: Sumi 5min Synergy WS intro: Sumi 5min. Subaru schedule: Koyama 5min. Synergy WS result: Sumi 10min. Discussion Yamada 15 min. Takahiro Sumi (Osaka U.) and JAXA Roman team 2021/3/5, Subaru Users Meeting FY2020 @online Nancy Grace Roman Space Telescope (May 2020 NASA renamed from WFIRST) Nancy G. Roman became NASA's first Chief of Astronomy in1959. known as the "Mother of Hubble" for her foundational role in planning the Hubble Space Telescope. Roman Space Telescope Solar Array Diameter: 2.4m Wavelength: λ=0.6-2.3μm Outer Barrel 2 Assembly Wide Field Inst. (WFI) (FOV：0.281deg. ) (OBA) Coronagraph Inst. (CGI)（tech demo） Sunshade Orbit: L2 Spacecraft Bus Mission life time: 5.3 years: 10years goal CGI WFI Serviceable Science (observation time): l Dark Energy/Modified Gravity(〜2.5yr) • High Latitude Survey (HLS)（galaxy distribution） • IaSNe survey l Exoplanets： • Microlensing exoplanet search (〜1.2yr) • Direct observation by coronagraph(〜0.3yr) l Guest Observer（25%,1.5yr） Roman Space Telescope Status l Advanced to phase C in Feb. 2020 l Mission Critical Design Review in Sept 2021 l Flight hardware - Telescope (L3Harris): Primary and secondary mirrors have been refigured, polished and coated; - Coronagraph relay optics polished and coated - Wide Field Instrument (GSFC/Ball) - Passed WFI CDR - Completed installation and alignment of all 18 engineering test unit (ETU) sensor chip assemblies (SCA) on the ETU mosaic plate - 17 out of 18 flight candidates SCAs in hand - Added new F213 filter (1.95-2.3) micron – now have imagining filter covering entire spectral range supported by mirrors/detectors 2021/3/5, Subaru Users Meeting FY2020 @online Roman Space Telescope Status Added new F213 filter (1.95-2.3) micron 2021/3/5, Subaru Users Meeting FY2020 @online Roman Space Telescope Status l Coronagraph (JPL) - Deformable mirror technology has been demonstrated - Two flight actuators in hand - CGI CDR April 2021 l Spacecraft (GSFC) - Procurement of flight subsystems well underway - Mechanical Hardware Engineering Development Units (EDUs) nearly complete l Ground system CDR July 2021 l On track for launch in mid 2020’s 2021/3/5, Subaru Users Meeting FY2020 @online Subaru-Roman Synergistic Observations Workshop IV Plan Synergistic observation utilizing the 100 nights of Subaru to enhance Roman science and enable new, joint science projects. Subaru-Roman Synergistic observation Steering Group: Toru Yamada (JAXA Roman Representative) Chair Takahiro Sumi (PI of the JAXA Roman study team) Yusei Koyama (Subaru Telescope Representative) Tadayuki Kodama (Liaison to the Subaru SAC) David Spergel (Roman WFI Adjutant Scientist) Julie McEnery (Roman Project Scientist) Jason Rhodes (Roman Deputy Project Scientist) Alice Shapley (RSIG representative) SOC: Daisuke Suzuki (Osaka U.) 2021/2/17–18, Subaru-Roman Synergistic Observations Workshop IV@online Synergy of Wide Field View (Credit: NAOJ) 1.5degree diameter Roman WFI 0.28deg2 Roman’s wide-band imaging has good synergy with Subaru’s multi-band capability. Japanese Contribution “Package” for Roman ■ JAXA Roman-J team (Team leader: T.Yamada, PI：Sumi） 1. Subaru-Roman Synergy Survey (100nights from 2025) 1. photo-z calibration (PFS etc.) 2. Narrow band filters (HSC etc.) 2016/11：Director of Subaru telescope and Subaru SAC、 agreed to the CoMMitMent ２．Contribution to Coronagraph Instrument ・Polarimetry capability ・coronagraph2020/03 mask substratesJAXA-NASA LOA signed. ３．Ka-band Data Downlink Station in Japan ４．Ground base microlensing data sharing（MOA） pre/concurrent Ground microlensing obs. with new 1.8m (PRIME) telescope JAXA Roman team members joined to SIT Roman 24 SIT member,、10 Domestic member 1. “COSMOLOGY WITH THE WFIRST HIGH LATITUDE SURVEY” (Chair: Olivier Dore ) Masahiro Takada (U.tokyo, IPMU), Hironao Miyatake (Nagoya U.), Tomomi Sunayama(Nagoya U.) 2. “OPTIMIZING THE WFIRST TYPE IA SUPERNOVA SURVEY” (Ryan Foley) Naoki Yasuda (U.tokyo, IPMU) Takashi Moriya (NAOJ),Yuji Urata (National Central University, Taipei) 3. "INVESTIGATING THE NATURE OF DARK ENERGY USING TYPE IA SUPERNOVAE WITH WFIRST-AFTA SPACE MISSION” (Saul Perlmutter) Nao Suzuki (U.tokyo, IPMU), Tomoki Morokuma (U.Tokyo, IoA) ------------------------ Exoplanet Microlensing 4. "PREPARING FOR THE WFIRST MICROLENSING SURVEY: SIMULATIONS, REQUIREMENTS, SURVEY STRATEGIES, AND PRECURSOR OBSERVATIONS” (Scott Gaudi) Takahiro Sumi (Osaka U.), Daisuke Suzuki (Osaka U.), Naoki Koshimoto (U.Tokyo), Kento Masuda (Osaka U.) ------------------------ Exoplanet Coronagraphs 5. “ OPTIMIZING WFIRST CORONAGRAPH SCIENCE”(Bruce Macintosh) Motohide Tamura (U. Tokyo/ABC), Taichi Uyama(Caltech/IPAC), Naoshi Murakami (Hokkaido U.) 6. "HARNESSING THE POWER OF THE WFIRST-CORONAGRAPH: A COORDINATED PLAN FOR EXOPLANET AND DISK SCIENCE”(Margaret Turnbull ) Taro Matsuo (Nagoya U.), Satoshi Ito(ISAS/JAXA) ------------------------ Guest Investigator (GI)/Guest Observer (GO) science 7. "WFIRST EXTRAGALACTIC POTENTIAL OBSERVATIONS (EXPO) SCIENCE INVESTIGATION TEAM” (Brant Robertson) Tadayuki Kodama (Tohoku U.), Takashi Moriya (NAOJ) Kimihiko Nakajima (NAOJ), Rhythm Shimakawa （NAOJ） 8. “WINGS: WFIRST INFRARED NEARBY GALAXY SURVEY” (Benjamin Williams) Masayuki Tanaka (NAOJ),Sakurako Okamoto (NAOJ) 9.“ARCHIVAL RESEARCH CAPABILITIES OF THE WFIRST DATA SET “(Alexander Szalay) Yusei Koyama (NAOJ) , Hisanori Furusawa(NAOJ),Masao Hayashi (NAOJ/Subaru), Tsuyoshi Terai (NAOJ/Subaru) 10.“COSMIC DAWN WITH WFIRST” (James Rhoads) Masami Ouchi (U. Tokyo, ICRR/NAOJ) Yuichi Harikane (NAOJ/UCL), Daisuke Yonetoku (Kanazawa U.) Masafusa Onoue（MPIA） 11. “RESOLVING THE MILKY WAY WITH WFIRST” (Jason KaliraiàJason Tumlison) Noriyuki Matsunaga (U.Tokyo IoA) Shogo Nishiyama (Miyagi Kyoiu U), Riku Urago (Kagoshima U.) The activities continue with New science teams Expected timeline. YEAR 2017 1st Workshop Collecting ideas, broad interest 2018 2nd Workshop Possible programs è summarized in WP 2019 3rd Workshop as a session in Possible programs in various Subaru 20th Meeting different science fields 2020 Preliminary proposal development of preliminary development ‘candidate programs’ 2021 4th Workshop NASA Roman Science Team(s) Solicitation 2022 TBD Consolidating the Program Front-loading program? 2023 TBD Proposal Planning, Teaming 2024 TBD Final Proposal Submission The proposal of the consolidated program will be reviewed by Subaru Advisory Committee 2025 TBD Scheduling White Paper of Synergistic observation Enabling Breakthrough Science with the Subaru EnablingTelescope Breakthroughand the Wide Field Science Infrared Surveywith the Telescope Subaru Telescope(WFIRST): and A White the paperWide forField Subaru Infrared and WFIRST Survey Communities Telescope (WFIRST): A White paper for Subaru April 25, 2019 2019/4/25 andEditors: WFIRST Jason Rhodes1 (Jet CommunitiesPropulsion Laboratory, California Institute of Technology), Takahiro Sumi2 (Osaka University) AlsoContents submitted to: US Decal survey Principal1. Executive EditorsSummary ................................: Jason Rhodes,................................ T.Sumi............................................................... 1 Executive2. Mission Capabilities Summary ................................: D. Spergel................................, T. Yamada.............................................................. 2 3. Exoplanet Microlensing......................................................................................................................... 5 4. Coronagraph Instrument (CGI) Support ................................................................................................ 8 http://www.ir.isas.jaxa.jp/WFIRST_Subaru_II/TALKS/WFI 5. Supernovae and Time Domain ............................................................................................................ 10 RST_Subaru_April25.pdf6. Deep Fields .......................................................................................................................................... 12 User7. Cosmology Name: ................................ wfirst ........................................................................................................... 17 Password:8. Nearby Galaxies subaru .................................................................................................................................. 19 9. Milky Way ........................................................................................................................................... 21 10. Solar System Science ....................................................................................................................... 23 11. General Guest Observer and Investigator Science: Keeping the Door Open to New Discoveries . 25 12. Future ProCess and Directions ........................................................................................................ 27 1. Executive Summary Authors: David Spergel (Flatiron Institute), Toru Yamada (JAXA) The Combination of joint WFIRST/Subaru observations have the potential to enable transformative science that cannot be done by either telescope alone. WFIRST will image the near-infrared sky to unprecedented depth and area. Subaru, with its wide field and unique instruments for both imaging and spectroscopy, is a superb complement. WFIRST and Subaru will also both be deploying
Recommended publications
  • A Review of Possible Planetary Atmospheres in the TRAPPIST-1 System

    A Review of Possible Planetary Atmospheres in the TRAPPIST-1 System

    Space Sci Rev (2020) 216:100 https://doi.org/10.1007/s11214-020-00719-1 A Review of Possible Planetary Atmospheres in the TRAPPIST-1 System Martin Turbet1 · Emeline Bolmont1 · Vincent Bourrier1 · Brice-Olivier Demory2 · Jérémy Leconte3 · James Owen4 · Eric T. Wolf5 Received: 14 January 2020 / Accepted: 4 July 2020 / Published online: 23 July 2020 © The Author(s) 2020 Abstract TRAPPIST-1 is a fantastic nearby (∼39.14 light years) planetary system made of at least seven transiting terrestrial-size, terrestrial-mass planets all receiving a moderate amount of irradiation. To date, this is the most observationally favourable system of po- tentially habitable planets known to exist. Since the announcement of the discovery of the TRAPPIST-1 planetary system in 2016, a growing number of techniques and approaches have been used and proposed to characterize its true nature. Here we have compiled a state- of-the-art overview of all the observational and theoretical constraints that have been ob- tained so far using these techniques and approaches. The goal is to get a better understanding of whether or not TRAPPIST-1 planets can have atmospheres, and if so, what they are made of. For this, we surveyed the literature on TRAPPIST-1 about topics as broad as irradiation environment, planet formation and migration, orbital stability, effects of tides and Transit Timing Variations, transit observations, stellar contamination, density measurements, and numerical climate and escape models. Each of these topics adds a brick to our understand- ing of the likely—or on the contrary unlikely—atmospheres of the seven known planets of the system.
  • Temperature Control for the Primary Mirror of Subaru Telescope Using the Data from 'Forecast for Mauna Kea Observatories'

    Temperature Control for the Primary Mirror of Subaru Telescope Using the Data from 'Forecast for Mauna Kea Observatories'

    Publ. Natl. Astron. Obs. Japan Vol. 7. 25–31 (2003) Temperature Control for the Primary Mirror of Subaru Telescope using the Data from ‘Forecast for Mauna Kea Observatories’ ∗ Akihiko MIYASHITA, Ryusuke OGASAWARA ,GeorgeMACARAYA†, and Noboru ITOH† (Received March 28, 2003) Abstract Based on the successful numerical weather forecasting performed by collaboration between the Mauna Kea Weather Center and Subaru Telescope, we developed a temperature control system for the primary mirror of the Subaru Telescope. Temperature forecast is accurate 80% in 2 degrees. After the start of operation, the temperature of the primary mirror controlled below 1 degree centigrade compared by the ambient night air temperature in over 70% probability. The effect of the temperature control for the improvement of the seeing of Subaru telescope seems to be moderately effective. The median of the seeing size of Subaru Telescope on May 2000 to March 2003 is 0.655 arcsec FWHM. We need further investigation as to whether the improvement is the result of our successful temperature control system of the primary mirror or the effect of the annual variation of seeing itself. Thus, we need a longer period of data for verification of the effectiveness of the temperature control. Key words: Subaru Telescope, Weather forecast, Seeing, Primary mirror, Temperature control. the actual night-time temperature over the entire night. 1. Introduction The predicted temperature by Mauna Kea Weather Center In order to obtain high quality images from optical- is used as a target temperature of the air-conditioning systems. infrared telescope, the heat generated by the instruments and After a preliminary test run of our method, it was found to equipment need to be removed.
  • Subaru Telescope: Current Instruments and Plans for Near-Future

    Subaru Telescope: Current Instruments and Plans for Near-Future

    Subaru Telescope: Current Instruments and Plans for Near-Future Ikuru Iwata (Subaru Telescope, NAOJ) New Development Group Scientist Photo by Enrico Sacchetti Current Subaru Instruments Primary Suprime-Cam FMOS NsOpt HDS NsIR AO188 IRCS CsOpt HiCIAO FOCAS SCExAO Kyoto 3DII CsIR MOIRCS COMICS Optical Instruments • FOCAS: Imaging, Multi-Object Spectroscopy, Polarization • FOV: 6’Φ, 0.10”/pix, R=250 - 7,500 (0.4” slit) • HDS: High-Dispersion Spectrograph • R=100,000 (0.38” slit), 0.14”/pix • Image Slicer: 0.3” x 5 opened in S11B • Suprime-Cam: Wide-Field Imaging • FOV: 34’ x 27’, 0.20”/pix • Kyoto 3D II: Three-Dimensional Spectroscopy • Fabry-Perot: FOV: 1.9‘x1.9’, 0.056”/pix, IFS: FOV: 3.4”x3.4”, 0.094”/pix Infrared Instruments • COMICS: Mid-IR Imaging and Spectroscopy • λ=8 - 25μm, FOV: 42”x32”, 0.13”/pix • FMOS: Near-IR Fiber Multi-Object Spectroscopy • 400 fibers, λ=0.9 - 1.8μm, FOV: 30’Φ, R= 500 & 2,200 • IRCS: Near-IR Imaging and Spectroscopy with AO • λ=0.9-5.5μm, FOV: 21” (20mas/pix), 54” (52mas/pix), R: 100-2,000 (grism), ~20,000 (echelle) • MOIRCS: Near-IR Wide-field Imaging and MOS • λ=0.9-2.5μm, FOV: 4’x7’, 0.12”/pix • AO188 / LGS: Adaptive Optics System with Laser Guide Star • HiCIAO: High-Contrast Coronagraph • λ=0.85-2.5μm, FOV: 20”x10” (DI, PDI), 5”x5” (SDI), 1e-5.5 contrast at r=1” Slide by H. Takami Two Outstanding Features among 8-10m Telescopes 1. Prime Focus 2. Good Image Quality Prime Focus Capability of Wide-Field Imaging and Spectroscopy Suprime-Cam FMOS • Fiber Multi-Object Spectrograph • 400 Fibers over 30’ Φ Field-of-View • 0.9 - 1.8 μm • OH Suppression with Mask Mirror FMOS Slide by N.
  • Globular Clusters and Galactic Nuclei

    Globular Clusters and Galactic Nuclei

    Scuola di Dottorato “Vito Volterra” Dottorato di Ricerca in Astronomia– XXIV ciclo Globular Clusters and Galactic Nuclei Thesis submitted to obtain the degree of Doctor of Philosophy (“Dottore di Ricerca”) in Astronomy by Alessandra Mastrobuono Battisti Program Coordinator Thesis Advisor Prof. Roberto Capuzzo Dolcetta Prof. Roberto Capuzzo Dolcetta Anno Accademico 2010-2011 ii Abstract Dynamical evolution plays a key role in shaping the current properties of star clus- ters and star cluster systems. We present the study of stellar dynamics both from a theoretical and numerical point of view. In particular we investigate this topic on different astrophysical scales, from the study of the orbital evolution and the mutual interaction of GCs in the Galactic central region to the evolution of GCs in the larger scale galactic potential. Globular Clusters (GCs), very old and massive star clusters, are ideal objects to explore many aspects of stellar dynamics and to investigate the dynamical and evolutionary mechanisms of their host galaxy. Almost every surveyed galaxy of sufficiently large mass has an associated group of GCs, i.e. a Globular Cluster System (GCS). The first part of this Thesis is devoted to the study of the evolution of GCSs in elliptical galaxies. Basing on the hypothesis that the GCS and stellar halo in a galaxy were born at the same time and, so, with the same density distribution, a logical consequence is that the presently observed difference may be due to evolution of the GCS. Actually, in this scenario, GCSs evolve due to various mechanisms, among which dynamical friction and tidal interaction with the galactic field are the most important.
  • The Mauna Kea Observatories Near-Infrared Filter Set. II. Specifications for a New JHKL!

    The Mauna Kea Observatories Near-Infrared Filter Set. II. Specifications for a New JHKL!

    Publications of the Astronomical Society of the Pacific, 114:180–186, 2002 February ᭧ 2002. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. The Mauna Kea Observatories Near-Infrared Filter Set. II. Specifications for a New JHKLЈMЈ Filter Set for Infrared Astronomy A. T. Tokunaga Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; [email protected] D. A. Simons Gemini Observatory, Northern Operations Center, 670 North A‘ohoku Place, Hilo, HI 96720; [email protected] and W. D. Vacca Max-Planck-Institut fu¨r extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany; [email protected] Received 2001 July 28; accepted 2001 October 17 ABSTRACT. We present a description of a new 1–5 mm filter set similar to the long-used JHKLM filter set derived from that of Johnson. The new Mauna Kea Observatories Near-Infrared filter set is designed to reduce background noise, improve photometric transformations from observatory to observatory, provide greater accuracy in extrapolating to zero air mass, and reduce the color dependence in the extinction coefficient in photometric reductions. We have also taken into account the requirements of adaptive optics in setting the flatness specification of the filters. A complete technical description is presented to facilitate the production of similar filters in the future. 1. INTRODUCTION baru Telescopes, all of the optical/infrared observatories at Mauna Kea are currently using these filters (NASA Infrared The rationale for a new set of infrared filters was presented Telescope Facility, United Kingdom Infrared Telescope, Canada- by Simons & Tokunaga (2002, hereafter Paper I).
  • Women of Goddard: Careers in Science, Technology, Engineering, and Mathematics

    Women of Goddard: Careers in Science, Technology, Engineering, and Mathematics

    Women of Goddard: Careers in Science, Technology, Engineering, and Mathematics Engineering, Technology, Careers in Science, of Goddard: Women National Aeronautics and Space Administration Goddard of Parkinson, Millar, Thaller Millar, Parkinson, Careers in Science Technology Engineering & Mathematics Women www.nasa.gov Women of Goddard NASA’s Goddard Space Flight Center IV&V, WV Goddard Institute for Space Studies, Greenbelt, Maryland, Main Campus Wallops Flight Facility, Virginia New York City Testing and Integration Facility, Greenbelt Home of Super Computing and Data Storage, Greenbelt GSFC’s new Sciences and Exploration Building, Greenbelt Women of Goddard: Careers in Science, Technology, Engineering, and Mathematics Editors: Claire L. Parkinson, Pamela S. Millar, and Michelle Thaller Graphics and Layout: Jay S. Friedlander In Association with: The Maryland Women’s Heritage Center (MWHC) NASA Goddard Space Flight Center, Greenbelt, Maryland, July 2011 Women of Goddard Careers in Foreword Science A century ago women in the United States could be schoolteachers and nurses but were largely excluded from the vast majority of other jobs that could Technology be classified as Science, Technology, Engineering, or Mathematics (STEM careers). Some inroads were fortuitously made during World Wars I and II, when because of Engineering the number of men engaged in fighting overseas it became essential that women fill in on jobs of all types on the home front. However, many of these inroads Mathematics were lost after the wars ended and the men
  • Progress in Nuclear Astrophysics of East and Southeast Asia

    Progress in Nuclear Astrophysics of East and Southeast Asia

    Aziz et al. AAPPS Bulletin (2021) 31:18 AAPPS Bulletin https://doi.org/10.1007/s43673-021-00018-z Review article Open Access Progress in nuclear astrophysics of east and southeast Asia Azni Abdul Aziz1, Nor Sofiah Ahmad2,S.Ahn3,WakoAoki4, Muruthujaya Bhuyan2, Ke-Jung Chen5,Gang Guo6,7,K.I.Hahn8,9, Toshitaka Kajino4,10,11*, Hasan Abu Kassim2,D.Kim12, Shigeru Kubono13,14, Motohiko Kusakabe11,15,A.Li15, Haining Li16,Z.H.Li17,W.P.Liu17*,Z.W.Liu18, Tohru Motobayashi14, Kuo-Chuan Pan19,20,21,22, T.-S. Park12, Jian-Rong Shi16,23, Xiaodong Tang24,25* ,W.Wang26,Liangjian Wen27, Meng-Ru Wu5,6, Hong-Liang Yan16,23 and Norhasliza Yusof2 Abstract Nuclear astrophysics is an interdisciplinary research field of nuclear physics and astrophysics, seeking for the answer to a question, how to understand the evolution of the universe with the nuclear processes which we learn. We review the research activities of nuclear astrophysics in east and southeast Asia which includes astronomy, experimental and theoretical nuclear physics, and astrophysics. Several hot topics such as the Li problems, critical nuclear reactions and properties in stars, properties of dense matter, r-process nucleosynthesis, and ν-process nucleosynthesis are chosen and discussed in further details. Some future Asian facilities, together with physics perspectives, are introduced. Keywords: Nuclear astrophysics, East and southeast Asia 1 Introduction • What are the nuclear reactions that drive the Nuclear astrophysics deals with astronomical phenomena evolution of stars and stellar explosions? involving atomic nuclei, and therefore, it is an interdis- ciplinary field that consists of astronomy, astrophysics, The research involves close collaboration among and nuclear physics.
  • Subaru Telescope —History, Active/Adaptive Optics, Instruments, and Scientific Achievements—

    Subaru Telescope —History, Active/Adaptive Optics, Instruments, and Scientific Achievements—

    No. 7] Proc. Jpn. Acad., Ser. B 97 (2021) 337 Review Subaru Telescope —History, active/adaptive optics, instruments, and scientific achievements— † By Masanori IYE*1, (Contributed by Masanori IYE, M.J.A.; Edited by Katsuhiko SATO, M.J.A.) Abstract: The Subaru Telescopea) is an 8.2 m optical/infrared telescope constructed during 1991–1999 and has been operational since 2000 on the summit area of Maunakea, Hawaii, by the National Astronomical Observatory of Japan (NAOJ). This paper reviews the history, key engineering issues, and selected scientific achievements of the Subaru Telescope. The active optics for a thin primary mirror was the design backbone of the telescope to deliver a high-imaging performance. Adaptive optics with a laser-facility to generate an artificial guide-star improved the telescope vision to its diffraction limit by cancelling any atmospheric turbulence effect in real time. Various observational instruments, especially the wide-field camera, have enabled unique observational studies. Selected scientific topics include studies on cosmic reionization, weak/strong gravitational lensing, cosmological parameters, primordial black holes, the dynamical/chemical evolution/interactions of galaxies, neutron star mergers, supernovae, exoplanets, proto-planetary disks, and outliers of the solar system. The last described are operational statistics, plans and a note concerning the culture-and-science issues in Hawaii. Keywords: active optics, adaptive optics, telescope, instruments, cosmology, exoplanets largest telescope in Asia and the sixth largest in the 1. Prehistory world. Jun Jugaku first identified a star with excess 1.1. Okayama 188 cm telescope. In 1953, UV as an optical counterpart of the X-ray source Yusuke Hagiwara,1 director of the Tokyo Astronom- Sco X-1.1) Sco X-1 was an unknown X-ray source ical Observatory, the University of Tokyo, empha- found at that time by observations using an X-ray sized in a lecture the importance of building a modern collimator instrument invented by Minoru Oda.2, 2) large telescope.
  • China's First Step Towards Probing the Expanding Universe and the Nature of Gravity Using a Space Borne Gravitational Wave

    China's First Step Towards Probing the Expanding Universe and the Nature of Gravity Using a Space Borne Gravitational Wave

    PERSPECTIVE https://doi.org/10.1038/s42005-021-00529-z OPEN China’s first step towards probing the expanding universe and the nature of gravity using a space borne gravitational wave antenna The Taiji Scientific Collaboration* In this perspective, we outline that a space borne gravitational wave detector network combining LISA and Taiji can be used to measure the Hubble constant with an uncertainty less than 0.5% in ten years, compared with the network of the ground based gravitational wave detectors which can measure the Hubble constant within a 2% uncertainty in the next five years by the standard siren method. Taiji is a Chinese space borne gravitational wave 1234567890():,; detection mission planned for launch in the early 2030 s. The pilot satellite mission Taiji-1 has been launched in August 2019 to verify the feasibility of Taiji. The results of a few tech- nologies tested on Taiji-1 are presented in this paper. he observation of gravitational waves (GWs) enables us to explore the Universe in more Tdetails than that is currently known. By testing the theory of general relativity, it can unveil the nature of gravity. In particular, a GW can be used to determine the Hubble constant by a standard siren method1,2. This method3 was first used by the Advanced LIGO4 and Virgo5 observatories when they discovered GW event GW1708176. Despite the degeneracy problem in the ground-based GW detectors, the Hubble constant can reach a precision of 2% after a 5-year observation with the network of the current surface GW detectors6, although LIGO’s O3 data have shown that the chance to detect electromagnetic (EM) counterpart might be a little optimistic7.
  • Arxiv:2108.11151V1 [Gr-Qc] 25 Aug 2021 Aee Siain 2,27]

    Arxiv:2108.11151V1 [Gr-Qc] 25 Aug 2021 Aee Siain 2,27]

    Alternative LISA-TAIJI networks: detectability to isotropic stochastic gravitational wave background Gang Wang1, ∗ and Wen-Biao Han1, 2, 3, † 1Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China 2Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310124, China 3School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China (Dated: August 26, 2021) In previous work [1], three TAIJI orbital deployments have been proposed to compose alternative LISA-TAIJI networks, TAIJIm (leading the Earth by 20◦ and −60◦ inclined with respect to ecliptic plane), TAIJIp (leading the Earth by 20◦ and +60◦ inclined), TAIJIc (colocated and coplanar with LISA) with respect to LISA mission (trailing the Earth by 20◦ and +60◦ inclined). And the LISA-TAIJIm network has been identified as the most capable configuration for massive black hole binary observation. In this work, we examine the performance of three networks to the stochastic gravitational wave background (SGWB) especially for the comparison of two eligible configurations, LISA-TAIJIm and LISA-TAIJIp. This investigation shows that the detectability of LISA-TAIJIm is competitive with the LISA-TAIJIp network for some specific SGWB spectral shapes. And the capability of LISA-TAIJIm is also identical to LISA-TAIJIp to separate the SGWB components by determining the parameters of signals. Considering the performances on SGWB and massive black hole binaries observations, the TAIJIm could be recognized as an optimal option to fulfill joint observations with LISA. I. INTRODUCTION In previous work, we proposed three TAIJI orbits to construct LISA-TAIJI networks and investigated their More than fifty gravitational wave (GW) events have performances on sky localizations for MBH binaries, con- been detected during the Advanced LIGO and Ad- straints on polarizations, and overlap reduction functions vanced Virgo observing runs O1-O3a, and all signals [1].
  • Space Activities 2019

    Space Activities 2019

    Space Activities in 2019 Jonathan McDowell [email protected] 2020 Jan 12 Rev 1.3 Contents Preface 3 1 Orbital Launch Attempts 3 1.1 Launch statistics by country . 3 1.2 Launch failures . 4 1.3 Commercial Launches . 4 2 Satellite Launch Statistics 6 2.1 Satellites of the major space powers, past 8 years . 6 2.2 Satellite ownership by country . 7 2.3 Satellite manufacture by country . 11 3 Scientific Space Programs 11 4 Military Space Activities 12 4.1 Military R&D . 12 4.2 Space surveillance . 12 4.3 Reconnaissance and Signals Intelligence . 13 4.4 Space Weapons . 13 5 Special Topics 13 5.1 The Indian antisatellite test and its implications . 13 5.2 Starlink . 19 5.3 Lightsail-2 . 24 5.4 Kosmos-2535/2536 . 25 5.5 Kosmos-2542/2543 . 29 5.6 Starliner . 29 5.7 OTV-5 and its illegal secret deployments . 32 5.8 TJS-3 . 33 6 Orbital Debris and Orbital Decay 35 6.1 Disposal of launch vehicle upper stages . 36 6.2 Orbituaries . 39 6.3 Retirements in the GEO belt . 42 6.4 Debris events . 43 7 Acknowledgements 43 Appendix 1: 2019 Orbital Launch Attempts 44 1 Appendix 2a: Satellite payloads launched in 2018 (Status end 2019) 46 Appendix 2b: Satellite payloads deployed in 2018 (Revised; Status end 2019) 55 Appendix 2c: Satellite payloads launched in 2019 63 Appendix 2d: Satellite payloads deployed in 2019 72 Rev 1.0 - Jan 02 Initial version Rev 1.1 - Jan 02 Fixed two incorrect values in tables 4a/4b Rev 1.2 - Jan 02 Minor typos fixed Rev 1.3 - Jan 12 Corrected RL10 variant, added K2491 debris event, more typos 2 Preface In this paper I present some statistics characterizing astronautical activity in calendar year 2019.
  • Mass and Hot Baryons in Massive Galaxy Clusters from Subaru Weak Lensing and Amiba SZE Observations

    Mass and Hot Baryons in Massive Galaxy Clusters from Subaru Weak Lensing and Amiba SZE Observations

    DRAFT VERSION OCTOBER 24, 2018 Preprint typeset using LATEX style emulateapj v. 08/22/09 MASS AND HOT BARYONS IN MASSIVE GALAXY CLUSTERS FROM SUBARU WEAK LENSING AND AMIBA SZE OBSERVATIONS 1 KEIICHI UMETSU2,3 , MARK BIRKINSHAW4,GUO-CHIN LIU2,5 , JIUN-HUEI PROTY WU6,3 ,ELINOR MEDEZINSKI7,TOM BROADHURST7, DORON LEMZE7,ADI ZITRIN7,PAUL T. P. HO2,8 ,CHIH-WEI LOCUTUS HUANG6,3 ,PATRICK M. KOCH2 ,YU-WEI LIAO6,3 ,KAI-YANG LIN2,6 ,SANDOR M. MOLNAR2, HIROAKI NISHIOKA2,FU-CHENG WANG6,3 ,PABLO ALTAMIRANO2,CHIA-HAO CHANG2,SHU-HAO CHANG2,SU-WEI CHANG2, MING-TANG CHEN2,CHIH-CHIANG HAN2 ,YAU-DE HUANG2,YUH-JING HWANG2 ,HOMIN JIANG2 , MICHAEL KESTEVEN9,DEREK Y. KUBO2 ,CHAO-TE LI2,PIERRE MARTIN-COCHER2,PETER OSHIRO2,PHILIPPE RAFFIN2 ,TASHUN WEI2,WARWICK WILSON9 Draft version October 24, 2018 ABSTRACT We present a multiwavelength analysis of a sample of four hot (TX > 8keV) X-ray galaxy clusters (A1689, A2261, A2142, and A2390) using joint AMiBA Sunyaev-Zel’dovich effect (SZE) and Subaru weak lensing observations, combined with published X-ray temperatures, to examine the distribution of mass and the intr- acluster medium (ICM) in massive cluster environments. Our observations show that A2261 is very similar to A1689 in terms of lensing properties. Many tangential arcs are visible around A2261, with an effective Einstein radius 40′′ (at z 1.5), which when combined with our weak lensing measurements implies a mass ∼ ∼ profile well fitted by an NFW model with a high concentration cvir 10, similar to A1689 and to other massive ∼ clusters. The cluster A2142 shows complex mass substructure, and displays a shallower profile (cvir 5), con- sistent with detailed X-ray observations which imply recent interaction.